Abstract:
We present a multiwavelength study of the NGC 281 complex which contains the young cluster IC 1590
at the center, using deep wide-field optical UBV Ic photometry, slitless spectroscopy along with archival
data sets in the near-infrared (NIR) and X-ray. The extent of IC 1590 is estimated to be ∼6.5 pc. The
cluster region shows a relatively small amount of differential reddening. The majority of the identified
young stellar objects (YSOs) are low mass PMS stars having age < 1−2 Myr and mass 0.5-3.5 M⊙. The
slope ($ \Gamma$) of the mass function for IC 1590, in the mass range 2<M/M⊙ ≤ 54, is found to be −1.11±0.15.
The slope of the K-band luminosity function (0.37±0.07) is similar to the average value (∼0.4) reported
for young clusters. The distribution of gas and dust obtained from the IRAS, CO and radio maps indicates
clumpy structures around the central cluster. The radial distribution of the young stellar objects, their
ages, (H −K) NIR-excess, and the fraction of classical T Tauri stars suggest triggered star formation
at the periphery of the cluster region. However, deeper optical, NIR and MIR observations are needed to
have a conclusive view of star formation scenario in the region. The properties of the Class 0/I and Class
II sources detected by using the Spitzer mid-infrared observations indicate that a majority of the Class II
sources are X-ray emitting stars, whereas X-ray emission is absent from the Class 0/I sources. The spatial
distribution of Class 0/I and Class II sources reveals the presence of three sub-clusters in the NGC 281
West region.
